We have combined ground-based optical and ISO spectra with
Hubble Space Telescope/Faint Object Spectrograph data
to study the emission line gas in the dwarf Seyfert 1
galaxy, NGC 4395. We have generated multicomponent
photoionization models, the predictions of which support the
suggestion that the emission-line gas is photoionized by a
strong source of non-thermal EUV radiation arising from the
core of the AGN. The narrow-line spectrum is well fitted by
a simple three-component model, while an additional
component was required to fit the broad lines. Models with
elemental abundances approximately 1/2 solar, with even
greater underabundance of nitrogen, provided the best fit to
the data, and are in general agreement with estimates from
studies of HII regions within NGC 4395. Much of the emission
line gas in the NLR appears to be dusty, and there may be a
significant amount of obscured gas, as evidenced by the
strength of IR fine structure lines such as [O~IV] 25.9\mu
and [S~IV] 10.5\mu. Assuming a central source luminosity
determined by a fit to the observed UV and X-ray continuum
fluxes, the models predict a covering factor of the emission
line gas greater than unity, indicating that the observed
continuum has been absorbed. The implications of the small
size and mass associated with this mini-AGN are discussed.